Abstract
In dust layer of a protoplanetary disk, the dust tends to revolve with the Kepler velocity. On the other hand the gas revolves with slower velocity than the Kepler velocity due to the pressure gradient. Thus shear flow occurs in the dust layer, depending on the dust density distribution. The shear instability could arise and then the flow would become turbulent. In this work, the dust gas tow fluid numerical simulations including the Coriolis force are performed in order to investigate the dust behavior in the shear-induced turbulence. We will indicate effect of the Coriolis force on the transit into turbulence and change of the dust density distribution.
